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TOI-5344 b: A Saturn-like planet orbiting a super-Solar metallicity M0 dwarf
We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0 dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habi...
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creator | Han, Te Robertson, Paul Kanodia, Shubham Cañas, Caleb Lin, Andrea S J Stefánsson, Guðmundur Libby-Roberts, Jessica E Larsen, Alexander Kobulnicky, Henry A Mahadevan, Suvrath Bender, Chad F Cochran, William D Endl, Michael Everett, Mark E Gupta, Arvind F Halverson, Samuel Hearty, Fred Monson, Andrew Ninan, Joe P Roy, Arpita Schwab, Christian Terrien, Ryan C |
description | We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0 dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (\(\rho = 0.80^{+0.17}_{-0.15}\ \text{g cm}^{-3}\)) with a planetary radius of \(9.7 \pm \ 0.5 \ \text{R}_{\oplus}\) (\(0.87 \pm \ 0.04 \ \text{R}_{\text{Jup}}\)) and a planetary mass of \(135^{+17}_{-18} \text{M}_{\oplus}\) (\(0.42^{+0.05}_{-0.06} \ \text{M}_{\text{Jup}}\)). It has an orbital period of \(3.792622 \pm 0.000010\) days and an orbital eccentricity of \(0.06^{+0.07}_{-0.04}\). We measure a high metallicity for TOI-5344 of [Fe/H] = \(0.48 \pm 0.12\), where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of non-giants (\(\lesssim 8\ \text{R}_{\oplus}\)). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats. |
doi_str_mv | 10.48550/arxiv.2310.20634 |
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TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (\(\rho = 0.80^{+0.17}_{-0.15}\ \text{g cm}^{-3}\)) with a planetary radius of \(9.7 \pm \ 0.5 \ \text{R}_{\oplus}\) (\(0.87 \pm \ 0.04 \ \text{R}_{\text{Jup}}\)) and a planetary mass of \(135^{+17}_{-18} \text{M}_{\oplus}\) (\(0.42^{+0.05}_{-0.06} \ \text{M}_{\text{Jup}}\)). It has an orbital period of \(3.792622 \pm 0.000010\) days and an orbital eccentricity of \(0.06^{+0.07}_{-0.04}\). We measure a high metallicity for TOI-5344 of [Fe/H] = \(0.48 \pm 0.12\), where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of non-giants (\(\lesssim 8\ \text{R}_{\oplus}\)). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.2310.20634</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Buttes ; Circumstellar habitable zone ; Deposition ; Extrasolar planets ; Metallicity ; Orbits ; Photometry ; Planet detection ; Planetary mass ; Radial velocity ; Red dwarf stars ; Transit</subject><ispartof>arXiv.org, 2023-11</ispartof><rights>2023. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). Notwithstanding the ProQuest Terms and Conditions, you may use this content in accordance with the terms of the License.</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktohtml>$$Uhttps://www.proquest.com/docview/2884924019?pq-origsite=primo$$EHTML$$P50$$Gproquest$$Hfree_for_read</linktohtml><link.rule.ids>778,782,25736,27908,36995,44573</link.rule.ids></links><search><creatorcontrib>Han, Te</creatorcontrib><creatorcontrib>Robertson, Paul</creatorcontrib><creatorcontrib>Kanodia, Shubham</creatorcontrib><creatorcontrib>Cañas, Caleb</creatorcontrib><creatorcontrib>Lin, Andrea S J</creatorcontrib><creatorcontrib>Stefánsson, Guðmundur</creatorcontrib><creatorcontrib>Libby-Roberts, Jessica E</creatorcontrib><creatorcontrib>Larsen, Alexander</creatorcontrib><creatorcontrib>Kobulnicky, Henry A</creatorcontrib><creatorcontrib>Mahadevan, Suvrath</creatorcontrib><creatorcontrib>Bender, Chad F</creatorcontrib><creatorcontrib>Cochran, William D</creatorcontrib><creatorcontrib>Endl, Michael</creatorcontrib><creatorcontrib>Everett, Mark E</creatorcontrib><creatorcontrib>Gupta, Arvind F</creatorcontrib><creatorcontrib>Halverson, Samuel</creatorcontrib><creatorcontrib>Hearty, Fred</creatorcontrib><creatorcontrib>Monson, Andrew</creatorcontrib><creatorcontrib>Ninan, Joe P</creatorcontrib><creatorcontrib>Roy, Arpita</creatorcontrib><creatorcontrib>Schwab, Christian</creatorcontrib><creatorcontrib>Terrien, Ryan C</creatorcontrib><title>TOI-5344 b: A Saturn-like planet orbiting a super-Solar metallicity M0 dwarf</title><title>arXiv.org</title><description>We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0 dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (\(\rho = 0.80^{+0.17}_{-0.15}\ \text{g cm}^{-3}\)) with a planetary radius of \(9.7 \pm \ 0.5 \ \text{R}_{\oplus}\) (\(0.87 \pm \ 0.04 \ \text{R}_{\text{Jup}}\)) and a planetary mass of \(135^{+17}_{-18} \text{M}_{\oplus}\) (\(0.42^{+0.05}_{-0.06} \ \text{M}_{\text{Jup}}\)). It has an orbital period of \(3.792622 \pm 0.000010\) days and an orbital eccentricity of \(0.06^{+0.07}_{-0.04}\). We measure a high metallicity for TOI-5344 of [Fe/H] = \(0.48 \pm 0.12\), where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of non-giants (\(\lesssim 8\ \text{R}_{\oplus}\)). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.</description><subject>Buttes</subject><subject>Circumstellar habitable zone</subject><subject>Deposition</subject><subject>Extrasolar planets</subject><subject>Metallicity</subject><subject>Orbits</subject><subject>Photometry</subject><subject>Planet detection</subject><subject>Planetary mass</subject><subject>Radial velocity</subject><subject>Red dwarf stars</subject><subject>Transit</subject><issn>2331-8422</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2023</creationdate><recordtype>article</recordtype><sourceid>PIMPY</sourceid><recordid>eNotjstqwzAUREWh0JDmA7oTdK1U1r2Kre5C6COQkkW8D9eyVJyqtivLffx9HdrVwHCYM4zdZHKJhdbyjuJ387lUMBVKrgAv2EwBZKJApa7YYhhOUkq1ypXWMGO7cr8VGhB5dc_X_EBpjK0IzZvjfaDWJd7FqklN-8qJD2Pvojh0gSJ_d4lCaGyTfviL5PUXRX_NLj2FwS3-c87Kx4dy8yx2-6ftZr0TZDQKU1vKamOcq6UC73NXgySyHnLQ3mUavCVlvNH-DBK63EvKsLIWoUCEObv9m-1j9zG6IR1P3fR6Mh5VUaBRKDMDv0aOTkg</recordid><startdate>20231107</startdate><enddate>20231107</enddate><creator>Han, Te</creator><creator>Robertson, Paul</creator><creator>Kanodia, Shubham</creator><creator>Cañas, Caleb</creator><creator>Lin, Andrea S J</creator><creator>Stefánsson, Guðmundur</creator><creator>Libby-Roberts, Jessica E</creator><creator>Larsen, Alexander</creator><creator>Kobulnicky, Henry A</creator><creator>Mahadevan, Suvrath</creator><creator>Bender, Chad F</creator><creator>Cochran, William D</creator><creator>Endl, Michael</creator><creator>Everett, Mark E</creator><creator>Gupta, Arvind F</creator><creator>Halverson, Samuel</creator><creator>Hearty, Fred</creator><creator>Monson, Andrew</creator><creator>Ninan, Joe P</creator><creator>Roy, Arpita</creator><creator>Schwab, Christian</creator><creator>Terrien, Ryan C</creator><general>Cornell University Library, arXiv.org</general><scope>8FE</scope><scope>8FG</scope><scope>ABJCF</scope><scope>ABUWG</scope><scope>AFKRA</scope><scope>AZQEC</scope><scope>BENPR</scope><scope>BGLVJ</scope><scope>CCPQU</scope><scope>DWQXO</scope><scope>HCIFZ</scope><scope>L6V</scope><scope>M7S</scope><scope>PIMPY</scope><scope>PQEST</scope><scope>PQQKQ</scope><scope>PQUKI</scope><scope>PRINS</scope><scope>PTHSS</scope></search><sort><creationdate>20231107</creationdate><title>TOI-5344 b: A Saturn-like planet orbiting a super-Solar metallicity M0 dwarf</title><author>Han, Te ; Robertson, Paul ; Kanodia, Shubham ; Cañas, Caleb ; Lin, Andrea S J ; Stefánsson, Guðmundur ; Libby-Roberts, Jessica E ; Larsen, Alexander ; Kobulnicky, Henry A ; Mahadevan, Suvrath ; Bender, Chad F ; Cochran, William D ; Endl, Michael ; Everett, Mark E ; Gupta, Arvind F ; Halverson, Samuel ; Hearty, Fred ; Monson, Andrew ; Ninan, Joe P ; Roy, Arpita ; Schwab, Christian ; Terrien, Ryan C</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-a954-9dca1d99eed023ff7ed30aacf3735fe153fca29f95fca1da4e7f0a14bcc438443</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2023</creationdate><topic>Buttes</topic><topic>Circumstellar habitable zone</topic><topic>Deposition</topic><topic>Extrasolar planets</topic><topic>Metallicity</topic><topic>Orbits</topic><topic>Photometry</topic><topic>Planet detection</topic><topic>Planetary mass</topic><topic>Radial velocity</topic><topic>Red dwarf stars</topic><topic>Transit</topic><toplevel>online_resources</toplevel><creatorcontrib>Han, Te</creatorcontrib><creatorcontrib>Robertson, Paul</creatorcontrib><creatorcontrib>Kanodia, Shubham</creatorcontrib><creatorcontrib>Cañas, Caleb</creatorcontrib><creatorcontrib>Lin, Andrea S J</creatorcontrib><creatorcontrib>Stefánsson, Guðmundur</creatorcontrib><creatorcontrib>Libby-Roberts, Jessica E</creatorcontrib><creatorcontrib>Larsen, Alexander</creatorcontrib><creatorcontrib>Kobulnicky, Henry A</creatorcontrib><creatorcontrib>Mahadevan, Suvrath</creatorcontrib><creatorcontrib>Bender, Chad F</creatorcontrib><creatorcontrib>Cochran, William D</creatorcontrib><creatorcontrib>Endl, Michael</creatorcontrib><creatorcontrib>Everett, Mark E</creatorcontrib><creatorcontrib>Gupta, Arvind F</creatorcontrib><creatorcontrib>Halverson, Samuel</creatorcontrib><creatorcontrib>Hearty, Fred</creatorcontrib><creatorcontrib>Monson, Andrew</creatorcontrib><creatorcontrib>Ninan, Joe P</creatorcontrib><creatorcontrib>Roy, Arpita</creatorcontrib><creatorcontrib>Schwab, Christian</creatorcontrib><creatorcontrib>Terrien, Ryan C</creatorcontrib><collection>ProQuest SciTech Collection</collection><collection>ProQuest Technology Collection</collection><collection>Materials Science & Engineering Collection</collection><collection>ProQuest Central (Alumni)</collection><collection>ProQuest Central</collection><collection>ProQuest Central Essentials</collection><collection>ProQuest Central</collection><collection>Technology Collection</collection><collection>ProQuest One Community College</collection><collection>ProQuest Central</collection><collection>SciTech Premium Collection</collection><collection>ProQuest Engineering Collection</collection><collection>Engineering Database</collection><collection>Publicly Available Content Database</collection><collection>ProQuest One Academic Eastern Edition (DO NOT USE)</collection><collection>ProQuest One Academic</collection><collection>ProQuest One Academic UKI Edition</collection><collection>ProQuest Central China</collection><collection>Engineering Collection</collection><jtitle>arXiv.org</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Han, Te</au><au>Robertson, Paul</au><au>Kanodia, Shubham</au><au>Cañas, Caleb</au><au>Lin, Andrea S J</au><au>Stefánsson, Guðmundur</au><au>Libby-Roberts, Jessica E</au><au>Larsen, Alexander</au><au>Kobulnicky, Henry A</au><au>Mahadevan, Suvrath</au><au>Bender, Chad F</au><au>Cochran, William D</au><au>Endl, Michael</au><au>Everett, Mark E</au><au>Gupta, Arvind F</au><au>Halverson, Samuel</au><au>Hearty, Fred</au><au>Monson, Andrew</au><au>Ninan, Joe P</au><au>Roy, Arpita</au><au>Schwab, Christian</au><au>Terrien, Ryan C</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>TOI-5344 b: A Saturn-like planet orbiting a super-Solar metallicity M0 dwarf</atitle><jtitle>arXiv.org</jtitle><date>2023-11-07</date><risdate>2023</risdate><eissn>2331-8422</eissn><abstract>We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0 dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (\(\rho = 0.80^{+0.17}_{-0.15}\ \text{g cm}^{-3}\)) with a planetary radius of \(9.7 \pm \ 0.5 \ \text{R}_{\oplus}\) (\(0.87 \pm \ 0.04 \ \text{R}_{\text{Jup}}\)) and a planetary mass of \(135^{+17}_{-18} \text{M}_{\oplus}\) (\(0.42^{+0.05}_{-0.06} \ \text{M}_{\text{Jup}}\)). It has an orbital period of \(3.792622 \pm 0.000010\) days and an orbital eccentricity of \(0.06^{+0.07}_{-0.04}\). We measure a high metallicity for TOI-5344 of [Fe/H] = \(0.48 \pm 0.12\), where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of non-giants (\(\lesssim 8\ \text{R}_{\oplus}\)). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.</abstract><cop>Ithaca</cop><pub>Cornell University Library, arXiv.org</pub><doi>10.48550/arxiv.2310.20634</doi><oa>free_for_read</oa></addata></record> |
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subjects | Buttes Circumstellar habitable zone Deposition Extrasolar planets Metallicity Orbits Photometry Planet detection Planetary mass Radial velocity Red dwarf stars Transit |
title | TOI-5344 b: A Saturn-like planet orbiting a super-Solar metallicity M0 dwarf |
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